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Comparing the Nucleosynthesis Parameters of s+r Stars and Ba Stars

Published online by Cambridge University Press:  01 April 2008

Wen-Yuan Cui ,
Dong-Nuan Cui  and
Bo Zhang
Wen-Yuan Cui
Affiliation:
Department of Physics, Hebei Normal University, 113 Yuhua Dong Road, Shijiazhuang 050016, P.R. China email: wenyuancui@126.com; zhangbo@hebtu.edu.cn
Dong-Nuan Cui
Affiliation:
Department of Physics, Hebei Normal University, 113 Yuhua Dong Road, Shijiazhuang 050016, P.R. China email: wenyuancui@126.com; zhangbo@hebtu.edu.cn
Bo Zhang
Affiliation:
Department of Physics, Hebei Normal University, 113 Yuhua Dong Road, Shijiazhuang 050016, P.R. China email: wenyuancui@126.com; zhangbo@hebtu.edu.cn
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Abstract

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In this paper, we use a parametric model of the asymptotic giant branch (AGB) stars, in which the 13C neutron source is activated in radiative conditions during the interpulse periods, to calculate the nucleosynthesis in 29 very metal-poor double-enhanced stars (i.e. s+r stars) and 26 barium stars (i.e. Ba stars), respectively. Through a statistical analyzing on the corresponding parameters obtained for the above stars, we get the possible conditions which the s+r stars formed in. We find that the value of neutron exposures of most s+r stars is greater than that of Ba stars. In the very metal-poor stars, the Ba stars stars should belong to the binary systems with large initial orbital separation, by comparing the s-process-component coefficient (Cs) values with those of s+r stars. For s+r stars, there is strong correlation between their Cs and Cr (r-process-component coefficient) but no correlation for Ba stars. This strongly confirms the possibility that the s+r stars should form through the accretion-induced collapse (AIC) or type 1.5 supernova mechanism.

Keywords

nucleosynthesisstars: abundancesAGB and post-AGB
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 113 - 114
Copyright
Copyright © International Astronomical Union 2008

References

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